• Source: Solar eclipse of February 14, 1934

      • A total solar eclipse occurred at the Moon's ascending node of orbit between Tuesday, February 13 and Wednesday, February 14, 1934, with a magnitude of 1.0321. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A total solar eclipse occurs when the Moon's apparent diameter is larger than the Sun's, blocking all direct sunlight, turning day into darkness. Totality occurs in a narrow path across Earth's surface, with the partial solar eclipse visible over a surrounding region thousands of kilometres wide. Occurring only 1.6 days after perigee (on February 12, 1934, at 11:20 UTC), the Moon's apparent diameter was smaller.
      Totality was visible from the Dutch East Indies (today's Indonesia), North Borneo (now belonging to Malaysia), and the South Seas Mandate of Japan (the part now belonging to FS Micronesia). A partial eclipse was visible for parts of East Asia, Southeast Asia, Australia, northern Oceania, Hawaii, and western North America.


      Eclipse details


      Shown below are two tables displaying details about this particular solar eclipse. The first table outlines times at which the moon's penumbra or umbra attains the specific parameter, and the second table describes various other parameters pertaining to this eclipse.


      Eclipse season



      This eclipse is part of an eclipse season, a period, roughly every six months, when eclipses occur. Only two (or occasionally three) eclipse seasons occur each year, and each season lasts about 35 days and repeats just short of six months (173 days) later; thus two full eclipse seasons always occur each year. Either two or three eclipses happen each eclipse season. In the sequence below, each eclipse is separated by a fortnight.


      Related eclipses




      = Eclipses in 1934

      =
      A partial lunar eclipse on January 30.
      A total solar eclipse on February 14.
      A partial lunar eclipse on July 26.
      An annular solar eclipse on August 10.


      = Metonic

      =
      Preceded by: Solar eclipse of April 28, 1930
      Followed by: Solar eclipse of December 2, 1937


      = Tzolkinex

      =
      Preceded by: Solar eclipse of January 3, 1927
      Followed by: Solar eclipse of March 27, 1941


      = Half-Saros

      =
      Preceded by: Lunar eclipse of February 8, 1925
      Followed by: Lunar eclipse of February 20, 1943


      = Tritos

      =
      Preceded by: Solar eclipse of March 17, 1923
      Followed by: Solar eclipse of January 14, 1945


      = Solar Saros 139

      =
      Preceded by: Solar eclipse of February 3, 1916
      Followed by: Solar eclipse of February 25, 1952


      = Inex

      =
      Preceded by: Solar eclipse of March 6, 1905
      Followed by: Solar eclipse of January 25, 1963


      = Triad

      =
      Preceded by: Solar eclipse of April 15, 1847
      Followed by: Solar eclipse of December 14, 2020


      = Solar eclipses of 1931–1935

      =
      This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.
      The partial solar eclipses on April 18, 1931 and October 11, 1931 occur in the previous lunar year eclipse set, and the solar eclipses on January 5, 1935 (partial), June 30, 1935 (partial), and December 25, 1935 (annular) occur in the next lunar year eclipse set.


      = Saros 139

      =
      This eclipse is a part of Saros series 139, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on May 17, 1501. It contains hybrid eclipses from August 11, 1627 through December 9, 1825 and total eclipses from December 21, 1843 through March 26, 2601. There are no annular eclipses in this set. The series ends at member 71 as a partial eclipse on July 3, 2763. Its eclipses are tabulated in three columns; every third eclipse in the same column is one exeligmos apart, so they all cast shadows over approximately the same parts of the Earth.
      The longest duration of totality will be produced by member 61 at 7 minutes, 29.22 seconds on July 16, 2186. This date is the longest solar eclipse computed between 4000 BC and AD 6000. All eclipses in this series occur at the Moon’s ascending node of orbit.


      = Metonic series

      =
      The metonic series repeats eclipses every 19 years (6939.69 days), lasting about 5 cycles. Eclipses occur in nearly the same calendar date. In addition, the octon subseries repeats 1/5 of that or every 3.8 years (1387.94 days). All eclipses in this table occur at the Moon's ascending node.


      = Tritos series

      =
      This eclipse is a part of a tritos cycle, repeating at alternating nodes every 135 synodic months (≈ 3986.63 days, or 11 years minus 1 month). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic month (period of perigee), but groupings of 3 tritos cycles (≈ 33 years minus 3 months) come close (≈ 434.044 anomalistic months), so eclipses are similar in these groupings.


      = Inex series

      =
      This eclipse is a part of the long period inex cycle, repeating at alternating nodes, every 358 synodic months (≈ 10,571.95 days, or 29 years minus 20 days). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic month (period of perigee). However, groupings of 3 inex cycles (≈ 87 years minus 2 months) comes close (≈ 1,151.02 anomalistic months), so eclipses are similar in these groupings.


      Notes




      References


      Earth visibility chart and eclipse statistics Eclipse Predictions by Fred Espenak, NASA/GSFC
      Google interactive map
      Besselian elements

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